Galaxy Sorting
... galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Interstellar ...
... galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Interstellar ...
Document
... • In a visual binary, you can see two stars. • However, for most binary stars, their separation is very small compared to their distance, and from Earth they appear to be a single point. • How do you observe these types of binaries? Use spectroscopy! ...
... • In a visual binary, you can see two stars. • However, for most binary stars, their separation is very small compared to their distance, and from Earth they appear to be a single point. • How do you observe these types of binaries? Use spectroscopy! ...
The star formation histories of two northern LMC fields
... the star formation rate in these fields, beginning approximately 2.5 Gyr ago, with the current metallicity in the region being Fe=H 20:38 ^ 0:10: The two fields have had very similar star formation rates until 200 Myr ago, at which point one shows a large increase. Key words: Magellanic Clouds ± ...
... the star formation rate in these fields, beginning approximately 2.5 Gyr ago, with the current metallicity in the region being Fe=H 20:38 ^ 0:10: The two fields have had very similar star formation rates until 200 Myr ago, at which point one shows a large increase. Key words: Magellanic Clouds ± ...
SciPoster_Jan2009
... the beginning of time (e.g., Yan et al. 2005). This dust was formed initially from massive short-lived stars such as Cassiopeia A (e.g., Rho 2008). Dust can also be formed from old, dying stars that used to be like our Sun. Dust found in molecular clouds is crucial to the star formation process beca ...
... the beginning of time (e.g., Yan et al. 2005). This dust was formed initially from massive short-lived stars such as Cassiopeia A (e.g., Rho 2008). Dust can also be formed from old, dying stars that used to be like our Sun. Dust found in molecular clouds is crucial to the star formation process beca ...
The Evolution of Stars - a More Detailed Picture (Chapter 8
... luminosity (Fig. 1). These are called Hayashi-tracks. In time, as the internal temperature continues to rise, ionisation is completed and the opacity drops. The convective zone recedes from the centre, and the star moves to higher effective temperatures. Slowly nuclear burning starts in the core. As ...
... luminosity (Fig. 1). These are called Hayashi-tracks. In time, as the internal temperature continues to rise, ionisation is completed and the opacity drops. The convective zone recedes from the centre, and the star moves to higher effective temperatures. Slowly nuclear burning starts in the core. As ...
Downloadable Full Text
... The UFD Reticulum II (Ret II) was recently discovered with Dark Energy Survey data12,13 and confirmed to be one of the most metal-poor galaxies known14. On 1-4 Oct 2015, we obtained high-resolution spectra of the nine brightest member stars in Ret II (see Table 1, Extended Data Figure 1). The abunda ...
... The UFD Reticulum II (Ret II) was recently discovered with Dark Energy Survey data12,13 and confirmed to be one of the most metal-poor galaxies known14. On 1-4 Oct 2015, we obtained high-resolution spectra of the nine brightest member stars in Ret II (see Table 1, Extended Data Figure 1). The abunda ...
script
... most familiar, outward to our Sun’s stellar neighbors, the other stars in our Milky Way galaxy, and into the universe of galaxies beyond. As we journey outward to distant galaxies we discover a surprising fact: the distant galaxies look much different than the galaxies closer to our Milky Way. Why i ...
... most familiar, outward to our Sun’s stellar neighbors, the other stars in our Milky Way galaxy, and into the universe of galaxies beyond. As we journey outward to distant galaxies we discover a surprising fact: the distant galaxies look much different than the galaxies closer to our Milky Way. Why i ...
PDF document
... has yet been definitely found at any redshift less than z = 0.12 over the 8.5 yr of the Swift mission to date25 . This suggests that either the rate of compact binary mergers is worryingly low for GW detection, or that most are not observed as bright SGRBs. The latter case could be understood if the ...
... has yet been definitely found at any redshift less than z = 0.12 over the 8.5 yr of the Swift mission to date25 . This suggests that either the rate of compact binary mergers is worryingly low for GW detection, or that most are not observed as bright SGRBs. The latter case could be understood if the ...
Ch 11a (Measuring Stars 10-28-10)
... Distance: If you know the parallax “p” (in arcseconds) you can calculate the distance “d” (in parsecs) d=1/p (1parsec= 3.26 lightyears) Apparent brightness: how bright a star looks in the sky The inverse-square Law: light from stars gets fainter as the inverse square of the distance (apparent bri ...
... Distance: If you know the parallax “p” (in arcseconds) you can calculate the distance “d” (in parsecs) d=1/p (1parsec= 3.26 lightyears) Apparent brightness: how bright a star looks in the sky The inverse-square Law: light from stars gets fainter as the inverse square of the distance (apparent bri ...
Document
... H-R diagrams are useful because they help astronomers categorize stars into groups: Main sequence stars, like the Sun, are in a very stable part of their life cycle. White dwarfs are hot and dim and cannot be seen without a telescope. Red giants are cool and bright and some can be seen witho ...
... H-R diagrams are useful because they help astronomers categorize stars into groups: Main sequence stars, like the Sun, are in a very stable part of their life cycle. White dwarfs are hot and dim and cannot be seen without a telescope. Red giants are cool and bright and some can be seen witho ...
The Strikingly Uniform, Highly Turbulent Interstellar Medium of the
... awarded 8.1h in bands 7 and 8 to study the red-shifted 157.7µm (2 P3/2 → 2 P1/2 ) fine-structure transition of ionized carbon, [C ii], and the underlying dust continuum emission in a sample of Hot DOGs spanning a range of redshifts and luminosities. Observations of W2246-0526, the first galaxy of th ...
... awarded 8.1h in bands 7 and 8 to study the red-shifted 157.7µm (2 P3/2 → 2 P1/2 ) fine-structure transition of ionized carbon, [C ii], and the underlying dust continuum emission in a sample of Hot DOGs spanning a range of redshifts and luminosities. Observations of W2246-0526, the first galaxy of th ...
The Extragalactic Group of MPE and USM
... of Massive Galaxies in the FORS Deep and GOODS South fields • Study evolution of galaxies with broadband deep U to K surveys. • LFs, Mass Functions, SFRs do not require spectroscopy but can be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter lumin ...
... of Massive Galaxies in the FORS Deep and GOODS South fields • Study evolution of galaxies with broadband deep U to K surveys. • LFs, Mass Functions, SFRs do not require spectroscopy but can be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter lumin ...
21_Testbank
... Answer: Starburst galaxies are filled with star-forming molecular clouds, which contain dust grains that absorb most of the visible light produced by the young stars. This radiation heats the dust grains to very high temperatures, and they re-emit all the absorbed energy as infrared light. 3) Explai ...
... Answer: Starburst galaxies are filled with star-forming molecular clouds, which contain dust grains that absorb most of the visible light produced by the young stars. This radiation heats the dust grains to very high temperatures, and they re-emit all the absorbed energy as infrared light. 3) Explai ...
The star Epsilon UMa, or more commonly known as Alioth
... Different stars have different apparent and absolute bolometric magnitudes. An apparent bolometric magnitude is a number scale invented by a Greek astronomer Hipparchus. This scale describes how bright a star appears in the night sky ranging from 1 for the brightest star to 6 for the dimmest star ab ...
... Different stars have different apparent and absolute bolometric magnitudes. An apparent bolometric magnitude is a number scale invented by a Greek astronomer Hipparchus. This scale describes how bright a star appears in the night sky ranging from 1 for the brightest star to 6 for the dimmest star ab ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... [Type Ia] and 100 times brighter than a typical core-collapse supernova,” state Howell and his 17 coauthors in a paper published in the December 20, 2013 issue of The Astrophysical Journal. For help in understanding the observations, Howell turned to computational astrophysicist Daniel Kasen, UC Ber ...
... [Type Ia] and 100 times brighter than a typical core-collapse supernova,” state Howell and his 17 coauthors in a paper published in the December 20, 2013 issue of The Astrophysical Journal. For help in understanding the observations, Howell turned to computational astrophysicist Daniel Kasen, UC Ber ...
Pulsating variable stars and the Hertzsprung
... showing a relationship between luminosity (or absolute magnitude) and stars' surface temperature (or spectral type). The bottom scale is ranging from high-temperature blue-white stars (left side of the diagram) to low-temperature red stars (right side). The position of a star on the diagram provides ...
... showing a relationship between luminosity (or absolute magnitude) and stars' surface temperature (or spectral type). The bottom scale is ranging from high-temperature blue-white stars (left side of the diagram) to low-temperature red stars (right side). The position of a star on the diagram provides ...
The Essential Cosmic Perspective, 6e
... 13) Based on the idea of "spaceship Earth," write one or two paragraphs explaining why it is not the case that we are "just sitting here." Answer: Far from just sitting still, we on Earth are moving relative to the Sun, planets, stars, and even other galaxies. The rotation of Earth causes the most ...
... 13) Based on the idea of "spaceship Earth," write one or two paragraphs explaining why it is not the case that we are "just sitting here." Answer: Far from just sitting still, we on Earth are moving relative to the Sun, planets, stars, and even other galaxies. The rotation of Earth causes the most ...
Beers_First_Stars_NIC_School
... times the solar mass. No clear evidence of supernovae from such supermassive stars has, however, yet been found in the chemical compositions of Milky Way stars. Here we report on an analysis of a very metal-poor star, SDSS J001820.5−093939.2, which possesses elemental-abundance ratios that differ si ...
... times the solar mass. No clear evidence of supernovae from such supermassive stars has, however, yet been found in the chemical compositions of Milky Way stars. Here we report on an analysis of a very metal-poor star, SDSS J001820.5−093939.2, which possesses elemental-abundance ratios that differ si ...
Stars, Galaxies, and the Universe Section 1
... • Binary stars are pairs of stars that revolve around each other and are held together by gravity. The center of mass, or barycenter, is somewhere between the two stars. • In star systems that have more than two stars, two stars may revolve rapidly around a common barycenter, while a third star revo ...
... • Binary stars are pairs of stars that revolve around each other and are held together by gravity. The center of mass, or barycenter, is somewhere between the two stars. • In star systems that have more than two stars, two stars may revolve rapidly around a common barycenter, while a third star revo ...
Presentation - Relativity Group
... • this, in turn, determines the number and relative strengths of absorption lines in the star’s spectrum • this fact was discovered by Cecilia Payne-Gaposchkin in 1925 ...
... • this, in turn, determines the number and relative strengths of absorption lines in the star’s spectrum • this fact was discovered by Cecilia Payne-Gaposchkin in 1925 ...
The HERMES GALAH survey: overview
... For large spirals like the Milky Way, the thick disk mass is typically about 10% of the thin disk, and its vertical scale height is about 1000 pc; the scale height of the thin disk is typically about 300 pc. Near the sun, the thick disk is more metal poor, although the abundance ranges of the thick ...
... For large spirals like the Milky Way, the thick disk mass is typically about 10% of the thin disk, and its vertical scale height is about 1000 pc; the scale height of the thin disk is typically about 300 pc. Near the sun, the thick disk is more metal poor, although the abundance ranges of the thick ...
The Milky Way - The Independent School
... Radio image of M 64: Central regions rotating backward! ...
... Radio image of M 64: Central regions rotating backward! ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.